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A pair-instability supernova is a type of supernova predicted to occur when pair production, the production of free electrons and positrons in the collision between atomic nuclei and energetic gamma rays, temporarily reduces the internal radiation pressure supporting a supermassive star's core against gravitational collapse. [1]
- Pulsational pair-instability supernova
A pulsational pair-instability supernova is a supernova...
- Pulsational pair-instability supernova
A pulsational pair-instability supernova is a supernova impostor event that generally occurs in stars at around 100 to 130 solar mass (M☉), as opposed to a typical pair-instability supernova which occurs in stars of 130 to 250 M☉.
In the 1980s, the term hypernova was used to describe a theoretical type of supernova now known as a pair-instability supernova. It referred to the extremely high energy of the explosion compared to typical core collapse supernovae.
30 Αυγ 2021 · The Wikipedia article on pair-instability supernovas (PISNs) doesn't seem to give a very good explanation of what causes a PISN. My understanding of the process it describes is this: Once the core gets hot enough, it starts producing gamma rays with enough energy to produce electron-positron pairs when they interact with atomic nuclei, although ...
7 Ιουν 2023 · The very massive first-generation stars with a mass range from 140 to 260 solar masses are predicted to enrich the early interstellar medium through pair-instability supernovae (PISNe)5.
15 Νοε 2007 · Here we report that the brightest supernovae in the modern Universe arise from collisions between shells of matter ejected by massive stars that undergo an interior instability arising from the...
3 Αυγ 2017 · In this chapter presents models of pair-instability supernovae (PISN). During core oxygen burning, models are rendered dynamically unstable by electron-positron pair production in an offcenter shell.
